X‐Ray States and Radio Emission in the Black Hole Candidate XTE J1550−564

Corbel, S.; Kaaret, Philip; Jain, R. K.; Bailyn, Charles D.; Fender, R. P.; Tomsick, J. A.; Kalemci, Emrah; McIntyre, Vince; Campbell-Wilson, D.; Miller, J. M.; McCollough, Michael L.

doi:10.1086/321364

Cited by 135 publications

(205 citation statements)

References 38 publications

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“…The magnetic field advected in the ADAF could be stronger, if the angular momentum carried by the outflows is properly considered, which leads to higher radial velocity. This is also consistent with relativistic jets always being associated with the low/hard state in X-ray binaries, while jets are switched off in the thermal state (Fender et al 1999Corbel et al 2001;Gallo et al 2003;) because jets are believed to be related to strong magnetic fields (Blandford & Znajek 1977;Blandford & Payne 1982). The viscosity parameter 0.1 a = corresponds to m 0.01, criṫ~w hich is roughly consistent with those derived from the transition from the thermal state to the low/hard state in some XRBs.…”

Section: ¢ = ¢supporting

confidence: 64%

An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

Cao

2016

ApJ

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We suggest a model of the advection-dominated accretion flow (ADAF) with magnetically driven outflows to explain the hysteretic state transition observed in X-ray binaries (XRBs). The transition from a thin disk to an ADAF occurs when the mass accretion rate is below a critical value. The critical mass accretion rate for the ADAF can be estimated by equating the equilibration timescale to the accretion timescale of the ADAF, which is sensitive to its radial velocity. The radial velocity of thin disks is very small, which leads to the advection of the external field in thin disks becoming very inefficient. ADAFs are present in the low/hard states of XRBs, and their radial velocity is large compared with the thin disk. The external field can be dragged inward efficiently by the ADAF, so a strong large-scale magnetic field threading the ADAF can be formed, which may accelerate a fraction of gas in the ADAF into the outflows. Such outflows may carry away a large amount of angular momentum from the ADAF, which significantly increases the radial velocity of the ADAF. This leads to a high critical mass accretion rate, below which an ADAF with magnetic outflows can survive. Our calculations show that the critical luminosity of the ADAF with magnetic outflows can be one order of magnitude higher than that for a conventional ADAF, if the ratio of gas to magnetic pressure 4 b~in the disk. This can naturally explain the hysteretic state transition observed in XRBs.

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Section: ¢ = ¢supporting

confidence: 64%

An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

Cao

2016

ApJ

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“…Broad-band radio to optical spectral energy distribution of XTE J1550-564 at MJD 51665 (red squares) and 51697 (green triangles and blue diamonds). The radio data are taken from Corbel et al (2001) and the OIR data from Jain et al (2001b). We plot the blackbody with temperature and normalization as inferred from the light curves and the CMD.…”

Section: Oir -X-ray Relationmentioning

confidence: 99%

Colours of black holes: infrared flares from the hot accretion disc in XTE J1550–564

Poutanen

Veledina

Revnivtsev

2014

Monthly Notices of the Royal Astronomical Society

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Outbursts of the black hole (BH) X-ray binaries are dramatic events occurring in our Galaxy approximately once a year. They are detected by the X-ray telescopes and often monitored at longer wavelengths. We analyse the X-ray and optical/infrared (OIR) light-curves of the BH binary XTE J1550-564 during the 2000 outburst. By using the observed extreme colours as well as the characteristic decay time-scales of the OIR and X-ray light curves, we put strong constraints on the extinction towards the source. We accurately separate the contributions to the OIR flux of the irradiated accretion disc and a non-thermal component. We show that the OIR non-thermal component appears during the X-ray state transitions both during the rising and the decaying part of the outburst at nearly the same X-ray hardness but at luminosities differing by a factor of 3. The line marking the quenching/recovery of the non-thermal component at the X-ray hardness-flux diagram seems to coincide with the 'jet line' that marks the presence of the compact radio jet. The inferred spectral shape and the evolution of the non-thermal component during the outburst, however, are not consistent with the jet origin, but are naturally explained in terms of the hybrid hot flow scenario, where non-thermal electrons emit synchrotron radiation in the OIR band. This implies a close, possibly causal connection between the presence of the hot flow and the compact jet. We find that the non-thermal component is hardening during the hard state at the decaying stage of the outburst, which indicates that the acceleration efficiency is a steep function of radius at low accretion rate.

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“…Finally, for systems with the highest luminosities (L bol /L Edd ∼ >0.3), in which the accretion flow might take the form of a radiation pressure-dominated slim disk (Abramowicz et al 1988), the X-ray spectrum can be dominated by a very steep power-law component (the "very-high" or "SPL" state). The very-high state itself is radio-quiet, but transitions from the very-high to the high state may be accompanied by optically thin ejection events in the radio (e.g., Corbel et al 2001;Hannikainen et al 2001;.…”

Section: Physical Interpretationmentioning

confidence: 99%

The Radio Quiescence of Active Galaxies with High Accretion Rates

Greene

Ulvestad

2006

ApJ

106

110

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We present 6 cm Very Large Array observations of the Greene & Ho (2004) sample of 19 low-mass active galaxies with high accretion rates. This is one of the only studies of a uniform sample of narrow-line Seyfert 1 (NLS1) galaxies with such high sensitivity and resolution. Although we detect only one source, the entire sample is very radio-quiet down to strong limits. GH10 was found to have a radio power of 8.5 ×10 21 W Hz −1 , and a ratio R ≡ f 6cm / f 4400 of 2.8. The 3 σ upper limits for the remaining nondetections correspond to radio powers from 3 × 10 20 to 8 × 10 21 W Hz −1 and 0.47 < R < 9.9. Stacking all nondetections yields an even stronger upper limit of R ≤ 0.27. An assessment of existing observations in the literature confirms our finding that NLS1s are consistently radio-quiet, with a radio-loud fraction of 0%-6%, which is significantly lower than the 10%-20% observed in the general quasar population. By analogy with stellar-mass black holes, we argue that AGNs undergo a state transition at L bol /L Edd ≈ 0.01. Below this value a radiatively inefficient accretion flow effectively drives an outflow, which disappears when the flow turns into an optically thick, geometrically thin disk, or a radiation pressure-dominated slim disk at still higher L bol /L Edd .

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X‐Ray States and Radio Emission in the Black Hole Candidate XTE J1550−564

Cited by 135 publications

References 38 publications

An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

Colours of black holes: infrared flares from the hot accretion disc in XTE J1550–564

The Radio Quiescence of Active Galaxies with High Accretion Rates

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